Non-standard neutrino cosmology dilutes the lensing anomaly

Esteban, Ivan; Mena, Olga; Salvadó, Jordi

doi:10.48550/arxiv.2202.04656

Cited by 5 publications

(7 citation statements)

References 103 publications

(145 reference statements)

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“…Finally, when considering the purely phenomenological parameter A lens , a positive degeneracy is expected between the former parameter and m ν : an increase in the neutrino mass will imply a depletion in the CMB lensing signal, as neutrinos are hot relics which suppress structure formation at small scales. This reduction can be compensated by increasing the A lens parameter, which controls the amount of smoothing induced in the CMB peaks by lensing [29][30][31][32][33]77]. The last row of Tab.…”

Section: Results On the Sum Of Neutrino Massesmentioning

confidence: 99%

“…There are however some other (not so simple and straightforward) extensions of the ΛCDM model which could lead to larger departures from the baseline 95% CL upper bound of 0.09 eV. That would be the case of non-standard neutrino physics [9][10][11][12][13][14][15][16], exotic dark sectors [17][18][19][20][21], a mixed hot dark matter scenario [22][23][24][25][26][27][28], or a modified CMB lensing pattern, parameterized this case by A lens [29][30][31][32][33], among other possibilities.…”

Section: Introductionmentioning

confidence: 99%

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Model marginalized constraints on neutrino properties from cosmology

Valentino¹,

Gariazzo²,

Mena³

2022

Preprint

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We present robust, model-marginalized limits on both the total neutrino mass ( mν ) and abundances (N eff ) to minimize the role of parameterizations, priors and models when extracting neutrino properties from cosmology. The cosmological observations we consider are Cosmic Microwave Background temperature fluctuation and polarization measurements, Supernovae Ia luminosity distances, Baryon Acoustic Oscillation observations and determinations of the growth rate parameter from the Data Release 16 of the Sloan Digital Sky Survey IV. The degenerate neutrino mass spectrum (which implies the prior mν > 0) is weakly (moderately) preferred over the normal and inverted hierarchy possibilities, which imply the priors mν > 0.06 and mν > 0.1 eV respectively. Concerning the underlying cosmological model, the ΛCDM minimal scenario is almost always strongly preferred over the possible extensions explored here. The most constraining 95% CL bound on the total neutrino mass in the ΛCDM+ mν picture is mν < 0.087 eV. The parameter N eff is restricted to 3.08 ± 0.17 (68% CL) in the ΛCDM+N eff model. These limits barely change when considering the ΛCDM+ mν + N eff scenario. Given the robustness and the strong constraining power of the cosmological measurements employed here, the model-marginalized posteriors obtained considering a large spectra of non-minimal cosmologies are very close to the previous bounds, obtained within the ΛCDM framework in the degenerate neutrino mass spectrum. Future cosmological measurements may improve the current Bayesian evidence favouring the degenerate neutrino mass spectra, challenging therefore the consistency between cosmological neutrino mass bounds and oscillation neutrino measurements, and potentially suggesting a more complicated cosmological model and/or neutrino sector.

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Section: Results On the Sum Of Neutrino Massesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Model marginalized constraints on neutrino properties from cosmology

Valentino¹,

Gariazzo²,

Mena³

2022

Preprint

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“…We then derive the equations governing a fluid of DM particles in the non-relativistic limit. This limit is the one relevant for DM, although in principle our derivation could apply to relativistic fluids like neutrinos [40,41]. The relativistic expressions are provided in appendix A.…”

Section: Frameworkmentioning

confidence: 99%

Unveiling dark fifth forces with linear cosmology

Archidiacono

Castorina

Redigolo

et al. 2022

J. Cosmol. Astropart. Phys.

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We initiate the exploration of the cosmology of dark fifth forces: new forces acting solely on Dark Matter. We focus on long range interactions which lead to an effective violation of the Equivalence Principle on cosmological scales today. At the microscopic level, the dark fifth force can be realized by a light scalar with mass smaller than the Hubble constant today (≲ 10-33 eV) coupled to Dark Matter. We study the behavior of the background cosmology and linear perturbations in such a Universe. At the background level, the new force modifies the evolution of the Dark Matter energy density and thus the Hubble flow. At linear order, it modifies the growth of matter perturbations and generates relative density and velocity perturbations between Dark Matter and baryons that grow over time. We derive constraints from current CMB and BAO data, bounding the strength of the dark fifth force to be less than a percent of gravity. These are the strongest constraints to date. We present potential implications of this scenario for the Hubble tension and discuss how our results are modified if the light scalar mediator accounts for the observed density of the Dark Energy. Finally, we comment on the interplay between our constraints and searches for violations of the Equivalence Principle in the visible sector.

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“…by e.g. assuming a non-standard cosmology [95][96][97][98], neutrinos with strong non-standard interactions [99][100][101][102][103], neutrinos with a time-varying mass [104][105][106][107][108][109], or neutrinos with a modified distribution function [110,111].…”

Section: A Probe Of Early Cνb Overdensitymentioning

confidence: 99%